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Range of Phase Integral Values for Asteroids

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Range of Phase Integral Values for Asteroids EPSC Abstracts Vol. 11, EPSC2017-776, 2017 European Planetary Science Congress 2017 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2017 Range of phase integral values for asteroids V. G. Shevchenko (1,2), and I. N. Belskaya (1) (1) Astronomical Institute of V. N. Karazin Kharkiv National University, Kharkiv, Ukraine, (2) Department of Astronomy and Space Informatics of V. N. Karazin Kharkiv National University, Kharkiv, Ukraine, ([email protected] / Fax: +38-057-7005349) Abstract function for the S-type we have combined the data for the asteroids 1862 Apollo and 5535 Annefrank The values of the phase integral were determined for [10, 11]. We have obtained the value of q equal to the main asteroid composition types using brightness 0.44 by the numerical integration. Using the data for phase functions in the wide phase angle range from the C-type asteroid 253 Mathilda [8, 12] and for the space mission data. We found that the range of phase E-type asteroid 2867 Steins [13] we obtained q integral values for asteroids of different composition equals to 0.34 and 0.54, respectively. Note, that the is within 0.34-0.54 with an average value of 0.42. value of the phase integral q=0.26 of 253 Mathilda given in [8] is smaller compared to our determination. The published values of phase integrals q=0.40 for 1. Introduction the MU-type asteroid 21 Lutetia [7] and q=0.44 for The phase integral q is a main component for the V-type asteroid 4 Vesta [14] are close to the determination of the Bond albedo that enters into the values for the S-type asteroids. These data show that thermal equilibrium equation and used for analyzing the range of q for asteroids of different types is data obtained in the infrared wavelength range. within 0.34-0.54. The range is smaller as compared Different authors have obtained different estimations to values calculated using the G or G1 and G2 of the phase integral of asteroids. Morrison [1] used parameters [15]. We used the composite phase the value of phase integral q=0.6. Later the function of brightness for these asteroids (Fig. 1) to relationship between q and G parameter of the HG- determine an average value of the phase integral. function [2] was used in [3-5]. Similar relationship has been proposed between q and G1, G2 parameters of the HG1G2-function [6]. The estimations of phase integrals have been made for asteroids using numerical integration of the phase function of brightness from space mission data [7, 8]. Here we investigate how the phase integral depends on asteroid composition types. 2. Results The detailed observations of phase function of asteroid brightness have revealed their similarity within the same compositional types [9]. Based on the average G, G1 and G2 parameters for the main compositional types and the proposed relations between q and these parameters, the phase integral q lies in the range from 0.34 (low-albedo asteroids) to Figure 1: Composite magnitude phase function of 0.64 (high-albedo asteroids). For some asteroids the asteroids [7, 8, 10-13]. phase functions of brightness have been obtained in a wide region of phase angles which allow direct There are differences in magnitude behavior at small calculation of the phase integral. To obtain the phase and large phase angles, but these differences are substantially less than global brightness changes in [11] Newburn, R. L., Duxbury, T. C., Hanner, M., et al.: the range of phase angles of 0-180 deg. We have Phase curve and albedo of asteroid 5535 Annefrank. J. obtained the value of q=0.42 for the whole data set. Geophys. Res., Vol. 108, pp. 5117-5122, 2003. [12] Mottola, S., Sears, W. D., Erikson, A., et al.: The slow 3. Conclusions rotation of 253 Mathilde. Planet. Space Sci., Vol. 43, pp. 1609-1613, 1995. A range of the values of the phase integral for asteroids of different compositional types lies from [13] A’Hearn, M. F., Feaga, L. M., Bertaux, J.-L., et al.: 0.34 to 0.54 with an average value of q =0.42. These The far-ultraviolet albedo of Steins measured with Rosetta- values can be used for determination of the Bond ALICE. Planet. Space Sci., Vol. 58, pp. 1088−1096, 2010. albedo of asteroids. [14] Hicks, M. D., Buratti, B. J., Lawrence, K. J., et al.: Spectral diversity and photometric behavior of main-belt References and near-Earth vestoids and (4) Vesta: A study in [1] Morrison, D.: Asteroid sizes and albedos. Icarus, Vol. preparation for the Dawn encounter. Icarus, Vol. 235, pp. 31, pp. 185–220. 1977. 60–74, 2014. [2] Bowell, E., Hapke, B., Domingue, D., et al.: Application [15] Shevchenko, V. G., Belskaya, I. N., Muinonen, K., et of photometric models to asteroids. In Asteroids II. Tucson. al.: Asteroid observations at low phase angles. IV. Average Univ. Arizona Press. P. 524−556, 1989. parameters for the new H, G1, G2 magnitude system. Planet. Space Sci., Vol. 123, pp. 101−116, 2016. [3] Tedesco, E. F., Noah, P. V., Noah, M., Price, S. D.: The supplemental IRAS minor planets survey. Astron. J., Vol. 123, pp. 1056−1085, 2002. [4] Masiero, J. R., Mainzer, A. K., Grav, T., et al.: Main belt asteroids with WISE/ NEOWISE. I. Preliminary albedos and diameters. Astrophys. J., Vol. 741, p. 68, 2011. [5] Usui, F., Kuroda, D., Muller, T. G., et al.: Asteroid catalog using Akari: AKARI/IRC mid-infrared asteroid survey. Publ. Astron. Soc. Japan, Vol. 63, pp. 1117–1138, 2011. [6] Muinonen, K., Belskaya, I. N., Cellino, A., et al.: A three-parameter phase-curve function for asteroids. Icarus, Vol. 209, pp. 542–555, 2010. [7] Masoumzadeh, N., Boehnhardt, H., Li, J.-Y., et al.: Photometric analysis of Asteroid (21) Lutetia from Rosetta- OSIRIS images. Icarus, Vol. 257, pp. 239–250, 2015. [8] Clark, B. E., Veverka, J., Helfenstein, P., et al.: NEAR photometry of asteroid 253 Mathilde. Icarus, Vol. 140, pp. 53−65, 1999. [9] Belskaya, I. N., and Shevchenko, V. G.: Opposition effect of asteroids. Icarus, Vol. 146, pp. 490-499, 2000. [10] Harris, A. W., Young, J. W., Goguen, J., et al.: Photoelectric lightcurves of the asteroid 1862 Apollo. Icarus, Vol. 70, pp. 246-256, 1987. .
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